In the received spectrograms, the Moon's face appears to lie on it's side, with the left-to-right time axis (6 s/pix) during the fan-beam passage approximately oriented south to north. The most favourable transits appear when the moon reaches its most northern declination (28.5°), then the elevation at the transmitter site is higher (more signal), and the passage is more parallel to he fan beam plane, resulting in longer total duration (up to 7 minutes) and higher Doppler resolution.

The Doppler axis (set to 0.042 Hz/pix) is west ("left" on moon, higher frequency) to east (lower frequency). The total spread is about 3 Hz from edge to edge, mostly caused by the diurnal variation of the aspect angle (libration) due to Earth's rotation. The receiver is locked to an OCXO, providing better than 0.1 ppb stability. To preserve the possible time-Doppler resolution, the overall chirp has to be removed at least approximately by applying a quadratic phase term (-0.0165 Hz/s) before doing the Fourier transforms.

The spectrograms are shown in pairs, with vertical polarization in the left and horizontal in the right half. By evaluating the signal correlation between the two receiver channels and subtracting any possible noise correlation, the polarization state of the specular reflection was derived. It is shown here as the spatial orientation of the major axis (+-atan(|H/V|), 0° vertical, +-90° horizontal) and the circularity (derived from the phase shift between H and V, 0° linear, +-90° circular polarized). Purely co- and crosspolarized signals were then synthesized, using linear combinations with maximum- and minimum-signal weighting respectively. Despite its much lower overall SNR, the crosspolarized component produced definitely nicer images, lacking the bright central glare caused by specular reflection. Presumably due to ionospheric Faraday rotation and changing electron contents, the received polarisation state varied from day to day in an unpredictable way.

Using IrfanView, the geometrical distortion of the images was corrected heuristically by remapping in four steps:
1. resize to 100x100 pixels ellipse width and height (=> large axis at 45°),
2. rotate left by 45° (=> ellipse upright),
3. resize to 100x100 pixels (=> circle),
4. rotate left by 30°...60° (=> north up).
The resulting crosspolarized image is shown as the rightmost picture for each day of observation.